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Observations indicate that the dispersal of protoplanetary discs in starclusters occurs on time scales of about 5 Myr. Several processes are thought tobe responsible for this disc dispersal. Here we compare two of these processes:dynamical encounters and interaction with the interstellar medium, whichincludes face-on accretion and ram pressure stripping. We perform simulationsof embedded star clusters with parameterisations for both processes todetermine the environment in which either of these processes is dominant. Wefind that face-on accretion, including ram pressure stripping, is the dominantdisc truncation process if the fraction of the total cluster mass in stars is$\lesssim 30\,\%$ regardless of the cluster mass and radius. Dynamicalencounters require stellar densities $\gtrsim 10^4$ pc$^{-3}$ combined with amass fraction in stars of $\approx 90\,\%$ to become the dominant process. Ourresults show that during the embedded phase of the cluster, the truncation ofthe discs is dominated by face-on accretion and dynamical encounters becomedominant when the intra-cluster gas has been expelled. As a result of face-onaccretion the protoplanetary discs become compact and their surface densityincreases. In contrast, dynamical encounters lead to discs that are lessmassive and remain larger.

Disc truncation in embedded star clusters: Dynamical encounters versus face-on accretion